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We present the results from a multiwavelength analysis of LS II+34 26, recently identified as a low mass post-AGB star and not a massive population I B-type star, as previously thought. We confirm that the central star is a carbon-poor post-AGB star surrounded by a very low excitation and compact nebula. Spectroscopic monitoring carried out since

We present a new integral field spectroscopic dataset of the central part of the Orion Nebula (M 42), observed with the MUSE instrument at the ESO VLT. We reduced the data with the public MUSE pipeline. The output products are two FITS cubes with a spatial size of ~5.´9×4.´9 (corresponding to ~0.76 × 0.63 pc2) and a contiguous wavelength coverage

We have compiled all the available optical B band data on OJ287, between 1890 and 1991. Using this data we have found a period of 11.6 +/- 0.5 yr for the outbursts in OJ 287. This value is in good agreement with the period of 11.65 yr between outbursts and 11.05 yr between minima found previously by Sillanpaa et al. (1988), using V-band data. Based

AutoFib2, the prime focus, multi-object spectrograph of the WHT, was recently upgraded with the installation of the Small Fibre Module. This allows to reach a fainter limiting magnitude and to observe a larger number of objects than with the previous large fibres.

We have developed a new stellar population synthesis model designed to study early-type galaxies. It provides optical and near-infrared colors, and line indices for 25 absorption lines. It can synthesize single age, single metallicity stellar populations, or follow the galaxy through its evolution from an initial gas cloud to the present time. The